中国科学院机构知识库网格系统: 检索

Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud 期刊论文 OAI收割
ASTROPHYSICAL JOURNAL, 2022, 卷号: 938, 期号: 2, 页码: 149
作者: Hou, X.; Ge, M. Y.; Ji, L.; Zhang, S. N.; You, Y.

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收藏 | 浏览/下载：5/0 | 提交时间：2023/11/09

Spectral and Timing Analysis of the Black Hole Transient MAXI J1631-479 During its 2019 Outburst Observed with Insight-HXMT 期刊论文 OAI收割
RESEARCH IN ASTRONOMY AND ASTROPHYSICS, 2022, 卷号: 22, 期号: 11, 页码: 115002
作者: Fu, Yu-Cong; Song, L. M.; Ding, G. Q.; Zhang, S. N.; Qu, J. L.

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收藏 | 浏览/下载：4/0 | 提交时间：2023/11/10

accretion accretion disks stars: black holes X-rays: binaries

The spectral-timing analysis of Cygnus X-1 with Insight-HXMT 期刊论文 OAI收割
ASTRONOMY & ASTROPHYSICS, 2022, 卷号: 666, 页码: A172
作者: Zhou, M; Grinberg, V; Bu, QC; Santangelo, A; Cangemi, F

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收藏 | 浏览/下载：3/0 | 提交时间：2023/11/09

X-rays binaries accretion accretion disks X-rays individuals Cygnus X-1 stars black holes

Synchronous X-ray/Optical QPOs from the Black Hole LMXB MAXI J1820+070 期刊论文 OAI收割
Monthly Notices of the Royal Astronomical Society, 2021
作者: HXMT

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收藏 | 浏览/下载：42/0 | 提交时间：2022/02/08

black hole physics Low Mass X-ray Binaries accretion accretion discs stars: individual (MAXI J1820+070) Astrophysics - High Energy Astrophysical Phenomena Abstract: We present high-speed optical photometry from SAAO and SALT on the black hole LMXB MAXI J1820+070 (ASSASN-18ey), some of it simultaneous with NICER, Swift and Insight-HXMT X-ray coverage. We detect optical Quasi-Periodic Oscillations (QPOs) that move to higher frequencies as the outburst progresses, tracking both the frequency and evolution of similar X-ray QPOs previously reported. Correlated X-ray/optical data reveal a complex pattern of lags, including an anti-correlation and a sub-second lag that evolve over the first few weeks of outburst. They also show correlated components separated by a lag equal to the QPO period roughly centered on zero lag, implying that the inter-band variability is strongly and consistently affected by these QPOs at a constant phase lag of roughly ±Ю The synchronisation of X-ray and optical QPOs indicates that they must be produced in regions physically very close to each other we thus propose that they can be explained by a precessing jet model, based on analogies with V404 Cyg and MAXI J1348-630.

The braking index of PSR B0540-69 and the associated pulsar wind nebula emission after spin-down rate transition 期刊论文 OAI收割
Monthly Notices of the Royal Astronomical Society, 2020, 卷号: 494, 页码: 1865-1870
作者: HXMT

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stars: magnetic field stars: neutron pulsars: general Astrophysics - High Energy Astrophysical Phenomena Abstract: In 2011 December, PSR B054-69 experienced a spin-down rate transition (SRT), after which the spin-down power of the pulsar increased by $\sim 36{{\ \rm per\ cent}}$. About 1000 d after the SRT, the X-ray luminosity of the associated pulsar wind nebula (PWN) was found to brighten by $32\pm 8{{\ \rm per\ cent}}$. After the SRT, the braking index n of PSR B0540-69 changes from n = 2.12 to 0.03 and then keeps this value for about five years before rising to n = 0.9 in the following years. We find that most of the current models have difficulties in explaining the measured braking index. One exceptive model of the braking index evolution is the increasing dipole magnetic field of PSR B0540-69. We suggest that the field increase may result from some instabilities within the pulsar core that enhance the poloidal component at the price of toroidal component of the magnetic field. The increasing dipole magnetic field will result in the X-ray brightening of the PWN. We fit the PWN X-ray light curve by two models: one assumes a constant magnetic field within the PWN during the brightening and the other assumes an enhanced magnetic field proportional to the energy density of the PWN. It appears that the two models fit the data well, though the later model seems to fit the data a bit better. This provides marginal observational evidence that magnetic field in the PWN is generated by the termination shock. Future high-quality and high-cadence data are required to draw a solid conclusion.

Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity 期刊论文 OAI收割
Monthly Notices of the Royal Astronomical Society, 2020, 卷号: 497, 页码: 5498-5506
作者: HXMT

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stars: neutron pulsars: individual: Swift J0243.6+6124 X-rays: binaries Astrophysics - High Energy Astrophysical Phenomena Abstract: Based on Insight-HXMT data, we report on the pulse fraction evolution during the 2017-2018 outburst of the newly discovered first Galactic ultraluminous X-ray (ULX) source Swift J0243.6+6124. The pulse fractions of 19 observation pairs selected in the rising and fading phases with similar luminosity are investigated. The results show a general trend of the pulse fraction increasing with luminosity and energy at supercritical luminosity. However, the relative strength of the pulsation between each pair evolves strongly with luminosity. The pulse fraction in the rising phase is larger at luminosity below 7.71 × 10³⁸ erg s^-1, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomenon is first confirmed by Insight-HXMT observations and we speculate that it may have relation with the radiation-pressure-dominated accretion disc.

Long-term evolutions of the cyclotron line energies in her x-1, vela x-1, and cen x-3 as observed with swift/bat 期刊论文 iSwitch采集
Monthly notices of the royal astronomical society, 2019, 卷号: 484, 期号: 3, 页码: 3797-3805
作者: Ji, L.; Staubert, R.; Ducci, L.; Santangelo, A.; Zhang, S.

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Radiation mechanisms: thermal Scattering Stars: magnetic field Stars: neutron X-rays: binaries X-rays: individual: her x-1, vela x-1, cen x-3

Long-term evolutions of the cyclotron line energies in her x-1, vela x-1, and cen x-3 as observed with swift/bat 期刊论文 iSwitch采集
Monthly notices of the royal astronomical society, 2019, 卷号: 484, 期号: 3, 页码: 3797-3805
作者:

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Radiation mechanisms: thermal Scattering Stars: magnetic field Stars: neutron X-rays: binaries X-rays: individual: her x-1, vela x-1, cen x-3

Unifying neutron star sub-populations in the supernova fallback accretion model 期刊论文 iSwitch采集
Research in astronomy and astrophysics, 2019, 卷号: 19, 期号: 3, 页码: 12
作者: Liu, Bai-Sheng; Li, Xiang-Dong

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Accretion, accretion disks Stars: neutron, evolution, rotation, magnetic field, magnetars Pulsars: general

Unifying neutron star sub-populations in the supernova fallback accretion model 期刊论文 iSwitch采集
Research in astronomy and astrophysics, 2019, 卷号: 19, 期号: 3, 页码: 12
作者: Liu, Bai-Sheng; Li, Xiang-Dong

收藏 | 浏览/下载：179/0 | 提交时间：2019/04/22

Accretion, accretion disks Stars: neutron, evolution, rotation, magnetic field, magnetars Pulsars: general